Spectroscopic diagnostics of coronal fan loops using EIS/Hinode and AIA/SDO
Abstract
We utilize spectroscopic and imaging data from the EIS/Hinode and the AIA/SDO to determine plasma and wave parameters along coronal fan loops. We determined the temperature along the loop lengths using the EM-loci method with EIS spectral lines and identified multi-thermal plasma components at temperatures ranging from 0.8-1.05, 1.2-1.4, and 1.6-1.8 MK. We further compared these temperature distributions along the loops with those derived from DEM analysis carried out using AIA coronal passbands. The multi-thermal nature of coronal fan loops can be well resolved using EIS spectroscopic data. We determined the density along the loop using the line-ratio method from the EIS Fe XII line pair. We found that density decreases slowly from the expected hydrostatic equilibrium. Our results demonstrate the multi-thermal nature of overdense loops, which can be well resolved with EIS spectroscopic data. We also determined the velocity amplitude of Alfvén waves from the non-thermal broadening of EIS Fe XII spectral line profiles. We further estimated the Alfvén wave energy flux in the corona by combining these parameters with the recently reported magnetic field strength of ≈200 G at the coronal footpoint of fan loops. The estimated Alfvén wave energy flux is ≈ 2× 107 erg cm−2 s−1, significantly higher than those reported in earlier studies, and can contribute to coronal losses due to radiation along the fan loops in the active region.
Related
- Heating of Solar Coronal Loops by Converging Unipolar Magnetic Flux: Evidence from SDO Observations and a Radiative MHD Simulation
- Fast and periodic propagating disturbances along coronal loops detected with EUI on board Solar Orbiter
- Volume Dependence of Helicity-based Eruption Diagnostics in Recurrent Coronal Jets
- Volume Dependence of Helicity-based Eruption Diagnostics in Recurrent Coronal Jets
- Coronal Green-Line Emission During a Solar Prominence Eruption: Spectroscopic Evidence of Its Correspondence with the EUV Late Phase
BibTeX
@misc{rawat2026spectroscopic,
title = {{Spectroscopic diagnostics of coronal fan loops using EIS/Hinode and AIA/SDO}},
author = {Ananya Rawat and Girjesh Gupta},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.05995},
eprint = {2611.05995},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.05995},
}
RIS
TY - UNPB
TI - Spectroscopic diagnostics of coronal fan loops using EIS/Hinode and AIA/SDO
AU - Ananya Rawat
AU - Girjesh Gupta
PY - 2026
DA - 2026/11/04
PB - arXiv
DO - 10.48550/arxiv.2611.05995
UR - https://arxiv.org/abs/2611.05995
AB - We utilize spectroscopic and imaging data from the EIS/Hinode and the AIA/SDO to determine plasma and wave parameters along coronal fan loops. We determined the temperature along the loop lengths using the EM-loci method with EIS spectral lines and identified multi-thermal plasma components at temperatures ranging from 0.8-1.05, 1.2-1.4, and 1.6-1.8 MK. We further compared these temperature distributions along the loops with those derived from DEM analysis carried out using AIA coronal passbands. The multi-thermal nature of coronal fan loops can be well resolved using EIS spectroscopic data. We determined the density along the loop using the line-ratio method from the EIS Fe XII line pair. We found that density decreases slowly from the expected hydrostatic equilibrium. Our results demonstrate the multi-thermal nature of overdense loops, which can be well resolved with EIS spectroscopic data. We also determined the velocity amplitude of Alfvén waves from the non-thermal broadening of EIS Fe XII spectral line profiles. We further estimated the Alfvén wave energy flux in the corona by combining these parameters with the recently reported magnetic field strength of ≈200 G at the coronal footpoint of fan loops. The estimated Alfvén wave energy flux is ≈ 2× 10^7 erg cm^−2 s^−1, significantly higher than those reported in earlier studies, and can contribute to coronal losses due to radiation along the fan loops in the active region.
ER -